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CO Multi-Line Imaging of Nearby Galaxies (COMING) IV. Overview Of
Publ. Astron. Soc. Japan (2018) 00(0), 1–33 1 doi: 10.1093/pasj/xxx000 CO Multi-line Imaging of Nearby Galaxies (COMING) IV. Overview of the Project Kazuo SORAI1, 2, 3, 4, 5, Nario KUNO4, 5, Kazuyuki MURAOKA6, Yusuke MIYAMOTO7, 8, Hiroyuki KANEKO7, Hiroyuki NAKANISHI9 , Naomasa NAKAI4, 5, 10, Kazuki YANAGITANI6 , Takahiro TANAKA4, Yuya SATO4, Dragan SALAK10, Michiko UMEI2 , Kana MOROKUMA-MATSUI7, 8, 11, 12, Naoko MATSUMOTO13, 14, Saeko UENO9, Hsi-An PAN15, Yuto NOMA10, Tsutomu, T. TAKEUCHI16 , Moe YODA16, Mayu KURODA6, Atsushi YASUDA4 , Yoshiyuki YAJIMA2 , Nagisa OI17, Shugo SHIBATA2, Masumichi SETA10, Yoshimasa WATANABE4, 5, 18, Shoichiro KITA4, Ryusei KOMATSUZAKI4 , Ayumi KAJIKAWA2, 3, Yu YASHIMA2, 3, Suchetha COORAY16 , Hiroyuki BAJI6 , Yoko SEGAWA2 , Takami TASHIRO2 , Miho TAKEDA6, Nozomi KISHIDA2 , Takuya HATAKEYAMA4 , Yuto TOMIYASU4 and Chey SAITA9 1Department of Physics, Faculty of Science, Hokkaido University, Kita 10 Nishi 8, Kita-ku, Sapporo 060-0810, Japan 2Department of Cosmosciences, Graduate School of Science, Hokkaido University, Kita 10 Nishi 8, Kita-ku, Sapporo 060-0810, Japan 3Department of Physics, School of Science, Hokkaido University, Kita 10 Nishi 8, Kita-ku, Sapporo 060-0810, Japan 4Division of Physics, Faculty of Pure and Applied Sciences, University of Tsukuba, 1-1-1 Tennodai, Tsukuba, Ibaraki 305-8571, Japan 5Tomonaga Center for the History of the Universe (TCHoU), University of Tsukuba, 1-1-1 Tennodai, Tsukuba, Ibaraki 305-8571, Japan 6Department of Physical Science, Osaka Prefecture University, Gakuen 1-1, -
Sunday October 19, 2014
Sunday October 19, 2014 Decided to use the Little Thompson Observatory’s telescopes tonight. I couldn’t connect to the 24”. Had connection failure issues. So I used the 18” f/14.2 and the 6” f/6 telescopes tonight. The 40mm eyepiece in 18” is 162x. The 22mm eyepiece in 6” is 41.5x. 7:00 PM. 68 degrees. Sky is clear. Wind is calm. Getting dark. Seeing and transparency Good. NGC 6929 7:27 PM 162x – Under a dim field star is this lopsided, faint, tiny oval glow. Glow goes to 2 o’clock from this star a tiny bit. Glow uniformly lit. NGC 6852 7:32 PM 162x – A brighter white star with very faint circular halo glow around it. With O3 see the halo a bit better and brighter. Star still prominent. NGC 6843 7:35 PM 162x – 7 very dim stars form this asterism in a small, rough circular pattern. NGC 6858 7:37 PM 162x – An asterism of 9 very dim stars in a diamond shape. NGC 6773 7:39 PM 162x – 5 stars form a box of 3 magnitudes with brightest still dim. PK 38-25.1 7:45 PM 162x – A stellar PN. A brighter white star. With O3, see a tiny bit of halo around it. It is small and hard to see. Looks like an out of focus star. Pal 11 7:49 PM 162x – With AV and waiting, see 3-4 very faint stars once in a while. In between a nice asterism pattern where picture shows it should be and where these 3-4 stars pop in. -
Expected Differences Between AGB Stars in the LMC and the SMC Due to Differences in Chemical Composition
New Views of the Magellanic Clouds fA U Symposium, Vol. 190, 1999 Y.-H. Chu, N.B. Suntzef], J.E. Hesser, and D.A. Bohlender, eds. Expected Differences between AGB Stars in the LMC and the SMC Due to Differences in Chemical Composition Ju. Frantsman Astronomical Institute, Latvian University, Raina Blvd. 19, Riga, LV-1586, LATVIA Abstract. Certain aspects of the AGB population, such as the relative number of M and N stars, the mass loss rates, and the initial masses of carbon- oxygen cores, depend on the initial heavy element abundance Z. I have calculated synthetic populations of AGB stars for different initial Z values taking into consideration the evolution of single and close binary stars. I present the results of population syntheses of AGB stars in clusters as a function of different initial chemical compositions. The relation for the tip luminosity of AGB stars versus cluster age as a function of Z is presented and is used to determine the ages for a number of clusters in the LMC and the SMC, including clusters with no previous age determinations. Population simulations show that for low heavy element abundance (Z = 0.001) few M stars are formed with respect to the number of carbon stars. However, the total number of all AGB stars in clusters is not affected by the initial chemical composition. As a result of the evolution of close binary components after the mass exchange, an increase in the range of limiting values of the thermal pulsing AGB star luminosities is expected. The difference between the maximum luminosity on the AGB of single star and the luminosity of a star after a mass exchange event in a close binary system may be as great as 1 magnitude for very young clusters. -
Astronomy Magazine Special Issue
γ ι ζ γ δ α κ β κ ε γ β ρ ε ζ υ α φ ψ ω χ α π χ φ γ ω ο ι δ κ α ξ υ λ τ μ β α σ θ ε β σ δ γ ψ λ ω σ η ν θ Aι must-have for all stargazers η δ μ NEW EDITION! ζ λ β ε η κ NGC 6664 NGC 6539 ε τ μ NGC 6712 α υ δ ζ M26 ν NGC 6649 ψ Struve 2325 ζ ξ ATLAS χ α NGC 6604 ξ ο ν ν SCUTUM M16 of the γ SERP β NGC 6605 γ V450 ξ η υ η NGC 6645 M17 φ θ M18 ζ ρ ρ1 π Barnard 92 ο χ σ M25 M24 STARS M23 ν β κ All-in-one introduction ALL NEW MAPS WITH: to the night sky 42,000 more stars (87,000 plotted down to magnitude 8.5) AND 150+ more deep-sky objects (more than 1,200 total) The Eagle Nebula (M16) combines a dark nebula and a star cluster. In 100+ this intense region of star formation, “pillars” form at the boundaries spectacular between hot and cold gas. You’ll find this object on Map 14, a celestial portion of which lies above. photos PLUS: How to observe star clusters, nebulae, and galaxies AS2-CV0610.indd 1 6/10/10 4:17 PM NEW EDITION! AtlAs Tour the night sky of the The staff of Astronomy magazine decided to This atlas presents produce its first star atlas in 2006. -
A Basic Requirement for Studying the Heavens Is Determining Where In
Abasic requirement for studying the heavens is determining where in the sky things are. To specify sky positions, astronomers have developed several coordinate systems. Each uses a coordinate grid projected on to the celestial sphere, in analogy to the geographic coordinate system used on the surface of the Earth. The coordinate systems differ only in their choice of the fundamental plane, which divides the sky into two equal hemispheres along a great circle (the fundamental plane of the geographic system is the Earth's equator) . Each coordinate system is named for its choice of fundamental plane. The equatorial coordinate system is probably the most widely used celestial coordinate system. It is also the one most closely related to the geographic coordinate system, because they use the same fun damental plane and the same poles. The projection of the Earth's equator onto the celestial sphere is called the celestial equator. Similarly, projecting the geographic poles on to the celest ial sphere defines the north and south celestial poles. However, there is an important difference between the equatorial and geographic coordinate systems: the geographic system is fixed to the Earth; it rotates as the Earth does . The equatorial system is fixed to the stars, so it appears to rotate across the sky with the stars, but of course it's really the Earth rotating under the fixed sky. The latitudinal (latitude-like) angle of the equatorial system is called declination (Dec for short) . It measures the angle of an object above or below the celestial equator. The longitud inal angle is called the right ascension (RA for short). -
The HST Key Project on the Extragalactic Distance Scale XIV
c The HST Key Project on the Extragalactic Distance Scale XIV. The Cepheids in NGC 1365' N. A. Silbermann,2 Paul Laura Ferrare~e,~Peter B. Stetson,5Barry F. Madore,' Robert C. Kennicutt, Jr.,3 Wendy L. ,Freedman,7.Jeremy R. i\/lould,' Fabio Bre~olin,~ HollandBrad E;. Gibson,' John A. Graham,"Mingsheng Han," John G. 'Based on observations with the NASA/ESA HubbleSpace Telescope obtained at the Space Telescope Science Institute, which is operated by AURA, Inc. under NASA Contract No. NAS5-265.55. 21nfrared Processing and Analysis Center, Jet Propulsion Laboratory, California Institute of Technology, MS 100-22, Pasadena, CA 91125 3Steward Observatory, University of Arizona, Tucson, A2 85721 4Hubble Fellow, California Institute of Technology, Pasadena, CA 91125 5Dominion Astrophysical Observatory, Victoria, British Columbia V8X 4M6 Canada 'NASA ExtragalacticDatabase, Infrared Processing and A4nalysis Center, California Institute of Technology, MS 100-22, Pasadena, CA 91125 70bservatories of the Carnegie Institution of Washington, Pa,sadena CA 91101 'Mount Stromlo and Siding Spring Observatories, Institute of Advanced Studies, ANU, ACT 2611 Australia 'Johns Hopkins University and Space Telescope Science Institute, Baltimore, MD 21218 "Dept. of Terrestrial Magnetism, Carnegie Institution of \Va.shington, Washington D.C. 20015 "University of Wisconsin, Madison, Wisconsin 53706 -- .j ~ ABSTRACT We report the detection of Clepheicl variable stars in the barred spiral galaxy NGC 1365, located in the Fornax cluster, using the Hubble Space Telescope Wide Field and Planetary Camera 2. Twelve V (F555W) and four I (F814W) epochs of observation were obtained. The two photometry packages, ALLFRAME and DoPHOT, were separately used to obtain profile-fitting photometry of all the stars in the HST field. -
And Ecclesiastical Cosmology
GSJ: VOLUME 6, ISSUE 3, MARCH 2018 101 GSJ: Volume 6, Issue 3, March 2018, Online: ISSN 2320-9186 www.globalscientificjournal.com DEMOLITION HUBBLE'S LAW, BIG BANG THE BASIS OF "MODERN" AND ECCLESIASTICAL COSMOLOGY Author: Weitter Duckss (Slavko Sedic) Zadar Croatia Pусскй Croatian „If two objects are represented by ball bearings and space-time by the stretching of a rubber sheet, the Doppler effect is caused by the rolling of ball bearings over the rubber sheet in order to achieve a particular motion. A cosmological red shift occurs when ball bearings get stuck on the sheet, which is stretched.“ Wikipedia OK, let's check that on our local group of galaxies (the table from my article „Where did the blue spectral shift inside the universe come from?“) galaxies, local groups Redshift km/s Blueshift km/s Sextans B (4.44 ± 0.23 Mly) 300 ± 0 Sextans A 324 ± 2 NGC 3109 403 ± 1 Tucana Dwarf 130 ± ? Leo I 285 ± 2 NGC 6822 -57 ± 2 Andromeda Galaxy -301 ± 1 Leo II (about 690,000 ly) 79 ± 1 Phoenix Dwarf 60 ± 30 SagDIG -79 ± 1 Aquarius Dwarf -141 ± 2 Wolf–Lundmark–Melotte -122 ± 2 Pisces Dwarf -287 ± 0 Antlia Dwarf 362 ± 0 Leo A 0.000067 (z) Pegasus Dwarf Spheroidal -354 ± 3 IC 10 -348 ± 1 NGC 185 -202 ± 3 Canes Venatici I ~ 31 GSJ© 2018 www.globalscientificjournal.com GSJ: VOLUME 6, ISSUE 3, MARCH 2018 102 Andromeda III -351 ± 9 Andromeda II -188 ± 3 Triangulum Galaxy -179 ± 3 Messier 110 -241 ± 3 NGC 147 (2.53 ± 0.11 Mly) -193 ± 3 Small Magellanic Cloud 0.000527 Large Magellanic Cloud - - M32 -200 ± 6 NGC 205 -241 ± 3 IC 1613 -234 ± 1 Carina Dwarf 230 ± 60 Sextans Dwarf 224 ± 2 Ursa Minor Dwarf (200 ± 30 kly) -247 ± 1 Draco Dwarf -292 ± 21 Cassiopeia Dwarf -307 ± 2 Ursa Major II Dwarf - 116 Leo IV 130 Leo V ( 585 kly) 173 Leo T -60 Bootes II -120 Pegasus Dwarf -183 ± 0 Sculptor Dwarf 110 ± 1 Etc. -
Publications OFTHK Astronomical Socik-N-Οκτπκ Pacific 101: 570-572, June 1989
Publications OFTHK Astronomical SociK-n-οκτπκ Pacific 101: 570-572, June 1989 A SURVEY FOR RR LYRAE VARIABLES IN FIVE SMALL MAGELLANIC CLOUD CLUSTERS ALISTAIR R. WALKER Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatories* Casilla 603, La Serena, Chile Received 1989 March 15 ABSTRACT Results are presented of a search for RR Lyrae variables in the SMC clusters NGC 121, Lindsay 1, Kron 3, Kron 7, and Kron 44. The techniques used rediscovered the four RR Lyraes in NGC 121, but no variables were found in the other clusters. It is concluded that RR Lyraes do not occur in SMC clusters younger than — 11 Gyr. Key words: star clusters-Magellanic Clouds-variable stars: RR Lyrae stars 1. Introduction Lindsay 1 but did not find any variables; however, the The Small Magellanic Cloud (SMC) contains a number majority of his plates were exposed in times of rather poor of populous clusters in the age range 3-12 Gyr, unlike seeing. A survey of several MC clusters for RR Lyraes was either the Galaxy or the Large Magellanic Cloud (LMC). made, using the Yale 1-m telescope and an image-tube Olszewski (1986) and Olszewski, Schommer, and camera, by Graham and Nemec (1984). They found many Aaronson (1987, henceforth OSA) point out that it should variables in old LMC clusters but none in the two SMC be possible to determine the age of the youngest cluster clusters blinked, NGC 339 and NGC 416. RR Lyraes by a suitable survey for the variables in the Since these surveys, color-magnitude diagrams candidate clusters. -
SCYON Issue 77
edited by Giovanni Carraro, Martin Netopil, and Ernst Paunzen https://www.univie.ac.at/scyon/ email: [email protected] The official Newsletter of the IAU Commission H4. SCYON Issue No. 77 September 30th, 2018 Dear Colleagues, This editorial is dedicated to an announcement by Amanda Karakas, the new President of the IAU Commission H4, which you can find on the next page. The current SCYON issue includes numerous paper abstracts, which cover a broad range in star cluster research. We also want to congratulate Maria Tiongco, who recently finished her PhD at the Indiana University. We wish her all the best for the future career! Furthermore, save the date for an upcoming conference in Bologna and register for one which takes place soon in Heidelberg. The SCYON editor team: Giovanni Carraro, Martin Netopil, and Ernst Paunzen CONTENTS About the Newsletter Abstracts of refereed papers . 3 SCYON publishes abstracts from any Star Forming Regions ..................3 area in astronomy, which are relevant to Galactic Open Clusters .................5 research on star clusters. We welcome all Galactic Globular Clusters .............8 kinds of submitted contributions (abstracts Clusters in the Magellanic clouds .......9 of refereed papers or conference proceedings, The most distant clusters .............11 PhD summaries, and general announcements Dynamical evolution - Simulations . 13 of e.g. conferences, databases, tools, etc.) Miscellaneous .........................16 Proceedings abstracts ....................17 The mission of this newsletter is to help Ph.D. (dissertation) summaries ...........18 all the researchers in the field with a quick Conferences and Announcements .........19 and efficient link to the scientific activity in the field. We encourage everybody to contribute to the new releases! New abstracts can be submitted at any time using the webform on the SCYON homepage. -
Star Clusters in Local Group Galaxies 3
Massive Stellar Clusters ASP Conference Series, Vol. XX, 2000 A. Lan¸con & C. Boily, eds. Star Clusters in Local Group Galaxies – Impact of Environment on Their Evolution and Survival Eva K. Grebel1,2 1University of Washington, Department of Astronomy, Box 351580, Seattle, WA 98195, USA 2Hubble Fellow Abstract. Star clusters are found in ∼40% of the Local Group galax- ies. Their properties are reviewed. The impact of galaxy environment on the evolution and survival of star clusters is discussed. Possible evi- dence for cluster formation triggered by galaxy interactions, gradients in cluster size, metallicity and stellar content with galactocentric radius and variations as a function of galaxy type are briefly summarized. 1. Introduction Star clusters in Local Group galaxies comprise a wide range of roughly coeval stellar agglomerates ranging from globular clusters to associations, from very metal-poor objects to clusters with solar and higher metallicity, and from ancient populations to embedded young clusters. Three basic types of such clusterings are observed: globular clusters, open clusters, and associations. 1.1. Globular Clusters Globular clusters are centrally concentrated, spherical systems with masses of 4.2 ∼< log M[M⊙] ∼< 6.6 and tidal radii ranging from ∼ 10 to ∼ 100 pc. They are bound, long-lived (∼>10 Gyr) objects whose lifetimes may extend to a Hubble arXiv:astro-ph/9912529v2 30 Dec 1999 time or beyond, though due to various efficient destruction mechanisms the presently observed globulars are likely just a lower limit of the initial number of globular clusters. Globular clusters have been observed in all known types of galaxies, but many of the less massive galaxies do not contain globular clusters. -
7.5 X 11.5.Threelines.P65
Cambridge University Press 978-0-521-19267-5 - Observing and Cataloguing Nebulae and Star Clusters: From Herschel to Dreyer’s New General Catalogue Wolfgang Steinicke Index More information Name index The dates of birth and death, if available, for all 545 people (astronomers, telescope makers etc.) listed here are given. The data are mainly taken from the standard work Biographischer Index der Astronomie (Dick, Brüggenthies 2005). Some information has been added by the author (this especially concerns living twentieth-century astronomers). Members of the families of Dreyer, Lord Rosse and other astronomers (as mentioned in the text) are not listed. For obituaries see the references; compare also the compilations presented by Newcomb–Engelmann (Kempf 1911), Mädler (1873), Bode (1813) and Rudolf Wolf (1890). Markings: bold = portrait; underline = short biography. Abbe, Cleveland (1838–1916), 222–23, As-Sufi, Abd-al-Rahman (903–986), 164, 183, 229, 256, 271, 295, 338–42, 466 15–16, 167, 441–42, 446, 449–50, 455, 344, 346, 348, 360, 364, 367, 369, 393, Abell, George Ogden (1927–1983), 47, 475, 516 395, 395, 396–404, 406, 410, 415, 248 Austin, Edward P. (1843–1906), 6, 82, 423–24, 436, 441, 446, 448, 450, 455, Abbott, Francis Preserved (1799–1883), 335, 337, 446, 450 458–59, 461–63, 470, 477, 481, 483, 517–19 Auwers, Georg Friedrich Julius Arthur v. 505–11, 513–14, 517, 520, 526, 533, Abney, William (1843–1920), 360 (1838–1915), 7, 10, 12, 14–15, 26–27, 540–42, 548–61 Adams, John Couch (1819–1892), 122, 47, 50–51, 61, 65, 68–69, 88, 92–93, -
(Ap) Mag Size Distance Rise Transit Set Gal NGC 6217 Arp 185 Umi
Herschel 400 Observing List, evening of 2015 Oct 15 at Cleveland, Ohio Sunset 17:49, Twilight ends 19:18, Twilight begins 05:07, Sunrise 06:36, Moon rise 09:51, Moon set 19:35 Completely dark from 19:35 to 05:07. Waxing Crescent Moon. All times local (EST). Listing All Classes visible above the perfect horizon and in twilight or moonlight before 23:59. Cls Primary ID Alternate ID Con RA (Ap) Dec (Ap) Mag Size Distance Rise Transit Set Gal NGC 6217 Arp 185 UMi 16h31m48.9s +78°10'18" 11.9 2.6'x 2.1' - 15:22 - Gal NGC 2655 Arp 225 Cam 08h57m35.6s +78°09'22" 11 4.5'x 2.8' - 7:46 - Gal NGC 3147 MCG 12-10-25 Dra 10h18m08.0s +73°19'01" 11.3 4.1'x 3.5' - 9:06 - PNe NGC 40 PN G120.0+09.8 Cep 00h13m59.3s +72°36'43" 10.7 1.0' 3700 ly - 23:03 - Gal NGC 2985 MCG 12-10-6 UMa 09h51m42.0s +72°12'01" 11.2 3.8'x 3.1' - 8:39 - Gal Cigar Galaxy M 82 UMa 09h57m06.5s +69°35'59" 9 9.3'x 4.4' 12.0 Mly - 8:45 - Gal NGC 1961 Arp 184 Cam 05h43m51.6s +69°22'44" 11.8 4.1'x 2.9' 180.0 Mly - 4:32 - Gal NGC 2787 MCG 12-9-39 UMa 09h20m40.5s +69°07'51" 11.6 3.2'x 1.8' - 8:09 - Gal NGC 3077 MCG 12-10-17 UMa 10h04m31.3s +68°39'09" 10.6 5.1'x 4.2' 12.0 Mly - 8:52 - Gal NGC 2976 MCG 11-12-25 UMa 09h48m29.2s +67°50'21" 10.8 6.0'x 3.1' 15.0 Mly - 8:36 - PNe Cat's Eye Nebula NGC 6543 Dra 17h58m31.7s +66°38'25" 8.3 22" 4400 ly - 16:49 - Open NGC 7142 Collinder 442 Cep 21h45m34.2s +65°51'16" 10 12.0' 5500 ly - 20:35 - Gal NGC 2403 MCG 11-10-7 Cam 07h38m20.9s +65°33'36" 8.8 20.0'x 10.0' 11.0 Mly - 6:26 - Open NGC 637 Collinder 17 Cas 01h44m15.4s +64°07'07" 7.3 3.0' 7000 ly - 0:33